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The crustal fraction of moment of inertia in neutron stars is calculatedusing $\beta$-equilibrated nuclear matter obtained from density dependent M3Yeffective interaction. The transition density, pressure and proton fraction atthe inner edge separating the liquid core from the solid crust of the neutronstars determined from the thermodynamic stability conditions are found to be$\rho_t=$ 0.0938 fm$^{-3}$, P$_t=$ 0.5006 MeV fm$^{-3}$ and $x_{p(t)}=$ 0.0308,respectively. The crustal fraction of the moment of inertia can be extractedfrom studying pulsar glitches and is most sensitive to the pressure as well asdensity at the transition from the crust to the core. These results forpressure and density at core-crust transition together with the observedminimum crustal fraction of the total moment of inertia provide a new limit forthe radius of the Vela pulsar: $R \geq 4.10 + 3.36 M/M_\odot$ kms.

Core-crust transition and crustal fraction of moment of inertia in neutron stars